Model atmospheres of irradiated exoplanets: The influence of stellar parameters, metallicity, and the C/O ratio
TLDR
In this paper, the properties of irradiated exoplanet atmospheres over a wide parameter range including metallicity, C/O ratio and host spectral type were studied. But the authors performed the calculations with their new Pressure-Temperature Iterator and Spectral Emission Calculator for Planetary Atmospheres (PETIT) code, assuming chemical equilibrium.Abstract:
Many parameters constraining the spectral appearance of exoplanets are still poorly understood. We therefore study the properties of irradiated exoplanet atmospheres over a wide parameter range including metallicity, C/O ratio and host spectral type. We calculate a grid of 1-d radiative-convective atmospheres and emission spectra. We perform the calculations with our new Pressure-Temperature Iterator and Spectral Emission Calculator for Planetary Atmospheres (PETIT) code, assuming chemical equilibrium. The atmospheric structures and spectra are made available online. We find that atmospheres of planets with C/O ratios $\sim$ 1 and $T_{\rm eff}$ $\gtrsim$ 1500 K can exhibit inversions due to heating by the alkalis because the main coolants CH$_4$, H$_2$O and HCN are depleted. Therefore, temperature inversions possibly occur without the presence of additional absorbers like TiO and VO. At low temperatures we find that the pressure level of the photosphere strongly influences whether the atmospheric opacity is dominated by either water (for low C/O) or methane (for high C/O), or both (regardless of the C/O). For hot, carbon-rich objects this pressure level governs whether the atmosphere is dominated by methane or HCN. Further we find that host stars of late spectral type lead to planetary atmospheres which have shallower, more isothermal temperature profiles. In agreement with prior work we find that for planets with $T_{\rm eff}$ $<$ 1750 K the transition between water or methane dominated spectra occurs at C/O $\sim$ 0.7, instead of $\sim$ 1, because condensation preferentially removes oxygen.read more
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Journal ArticleDOI
A chemical survey of exoplanets with ARIEL
Giovanna Tinetti,Pierre Drossart,Paul Eccleston,Paul Hartogh,A. Heske,Jérémy Leconte,Giuseppina Micela,Marc Ollivier,Göran Pilbratt,L. Puig,Diego Turrini,Bart Vandenbussche,Paulina Wolkenberg,Jean-Philippe Beaulieu,Lars A. Buchave,Martin Ferus,Matthew Joseph Griffin,Manuel Guedel,Kay Justtanont,Pierre Olivier Lagage,Pedro Machado,Giuseppe Malaguti,Michiel Min,Hans Ulrik Nørgaard-Nielsen,M. Rataj,Tom Ray,Ignasi Ribas,Mark R. Swain,Róbert Szabó,Stephanie C. Werner,Joanna K. Barstow,Matthew R. Burleigh,James Y-K. Cho,Vincent Coudé du Foresto,Athena Coustenis,Leen Decin,Thérèse Encrenaz,Marina Galand,Michaël Gillon,Ravit Helled,Juan Carlos Morales,Antonio García Muñoz,A. Moneti,Isabella Pagano,Enzo Pascale,Giuseppe Piccioni,D. J. Pinfield,Subhajit Sarkar,Franck Selsis,Jonathan Tennyson,Amaury H. M. J. Triaud,Olivia Venot,Ingo Waldmann,David Waltham,Gillian S. Wright,Jérôme Amiaux,Jean Louis Auguères,Michel Berthé,Naidu Bezawada,Georgia Bishop,Neil Bowles,Deirdre Coffey,Josep Colomé,Martin Crook,Pierre-Elie Crouzet,Vania Da Peppo,Isabel Escudero Sanz,Mauro Focardi,Martin Frericks,T. Hunt,R. Kohley,Kevin Middleton,Gianluca Morgante,Roland Ottensamer,Emanuele Pace,Chris Pearson,R. Stamper,Kate Symonds,Miriam Rengel,Etienne Renotte,Peter A. R. Ade,Laura Affer,Christophe Alard,Nicole F. Allard,Francesca Altieri,Y. André,C. Arena,Ioannis Argyriou,Alan D. Aylward,Cristian Baccani,Gáspár Á. Bakos,Marek Banaszkiewicz,M. J. Barlow,V. Batista,Giancarlo Bellucci,Serena Benatti,Pernelle Bernardi,Bruno Bézard,M. I. Blecka,Emeline Bolmont,Bertrand Bonfond,Rosaria Bonito,Aldo S. Bonomo,John Robert Brucato,Allan Sacha Brun,Ian Bryson,Waldemar Bujwan,Sarah L. Casewell,Bejamin Charnay,Cesare Cecchi Pestellini,Guo Chen,Angela Ciaravella,Riccardo Claudi,R. Cledassou,Mario Damasso,M. Damiano,Camilla Danielski,Pieter Deroo,Anna Maria Di Giorgio,Carsten Dominik,Vanessa Doublier,Simon Doyle,René Doyon,Benjamin Drummond,Bastien Duong,Stephen Anthony Eales,Billy Edwards,M. Farina,Ettore Flaccomio,Leigh N. Fletcher,François Forget,S. J. Fossey,Markus Fränz,Yuka Fujii,A. Garcia-Piquer,Walter Kieran Gear,Hervé Geoffray,Jean-Claude Gérard,Lluis Gesa,Haley Louise Gomez,Rafal Graczyk,Caitlin A. Griffith,Denis Grodent,M. G. Guarcello,Jacques Gustin,Keiko Hamano,Peter Charles Hargrave,Yann Hello,Kevin Heng,E. Herrero,Allan Hornstrup,Benoît Hubert,Shigeru Ida,Masahiro Ikoma,N. Iro,Patrick G. J. Irwin,Christopher Jarchow,Jean Jaubert,Hugh R. A. Jones,Queyrel Julien,Shingo Kameda,Franz Kerschbaum,Pierre Kervella,Tommi Koskinen,Matthijs Krijger,Norbert Krupp,M. Lafarga,Federico Landini,Emanuel Lellouch,Giuseppe Leto,A. Luntzer,Theresa Rank-Lüftinger,Antonio Maggio,Jesus Maldonado,Jean Pierre Maillard,Urs Mall,Jean Baptiste Marquette,Stéphane Mathis,Pierre F. L. Maxted,Taro Matsuo,Alexander S. Medvedev,Yamila Miguel,Vincent Minier,Giuseppe Morello,Alessandro Mura,Norio Narita,Valerio Nascimbeni,N. Nguyen Tong,Vladimiro Noce,Fabrizio Oliva,Enric Palle,Paul Palmer,Maurizio Pancrazzi,Andreas Papageorgiou,Vivien Parmentier,Manuel Perger,A. Petralia,Stefano Pezzuto,Raymond T. Pierrehumbert,Ignazio Pillitteri,Giampaolo Piotto,Giampaolo Pisano,Loredana Prisinzano,Aikaterini Radioti,Jean Michel Reess,Ladislav Rezac,Marco Rocchetto,A. Rosich,Nicoletta Sanna,Alexandre Santerne,Giorgio Savini,Gaetano Scandariato,Bruno Sicardy,Carles Sierra,Giuseppe Sindoni,Konrad Skup,Ignas Snellen,Mateusz Sobiecki,Lauriane Soret,Alessandro Sozzetti,Arnaud Stiepen,Antoine Strugarek,Jake Taylor,William Taylor,Luca Terenzi,Marcell Tessenyi,Angelos Tsiaras,C. Tucker,Diana Valencia,Gautam Vasisht,Allona Vazan,Francesc Vilardell,Sabrine Vinatier,Serena Viti,Rens Waters,Piotr Wawer,A. Wawrzaszek,Anthony Peter Whitworth,Yuk L. Yung,Sergey N. Yurchenko,Maria Rosa Zapatero Osorio,Robert T. Zellem,Tiziano Zingales,Frans Zwart +243 more
TL;DR: The ARIEL mission as mentioned in this paper was designed to observe a large number of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25-7.8 μm spectral range and multiple narrow-band photometry in the optical.
Journal ArticleDOI
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Journal ArticleDOI
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